白天非自发光天体目标探测技术的研究

本文讨论了在白天晴空背景下非自发光天体目标探测系统的探测极限、目标对比度及信噪比与目标特性、天空背景特性、光学系统参数和CCD参数之间的关系,重点讨论了光谱滤波技术对探测极限、对比度、信噪比的影响,数值仿真结果表明:光谱滤波技术可以将目标的光学对比度提高4——8倍,将目标的信噪比提高1.6——2.5倍,可将系统的极限探测星等提高0.4——0.7个目视星等。     

短波红外全天时自主天文导航技术展望

基于2微米全天巡天（2MASS）短波红外巡天点源星表,分别从白天可探测恒星分布、天空背景辐射与大气传输、传感器性能和光学系统视场大小等方面,分析了短波红外波段相对于可见光波段,在大气层内白天观星实现全天时天文导航的优势,并展望了其发展方向。     

一种GEO空间目标快速识别算法

由于GEO(地球同步轨道)空间目标相对背景恒星的视运动速度较慢,使用相邻帧图像差分的方法难以自动识别并跟踪目标。基于Lucas-Kanade算法,使用在全图所有星像的邻域开窗,计算统计波门内星像的移动速度,根据目标的运动特征给定全局阈值判别的方法,实现了相邻帧短曝光图像间的GEO目标自动识别与跟踪。仿真实验表明,该算法稳健可靠,星像位移计算精度为10-3,计算时间快于0.1s,在观测数据的实时处理中有较大的应用价值。     

白天天空背景亮度仿真研究

天空背景辐射严重影响光电系统对空间目标的探测跟踪能力，克服背景辐射干扰是解决白天目标探测跟踪的重要工作。本文描述了通过求解大气辐射传输方程，仿真计算白天天空背景亮度的方法，分析了不同太阳天项角、观测方向以及不同大气光学厚度条件下天空背景亮度。     

近地空间全天时星敏感器技术现状及发展综述

星敏感器是一种以恒星为参考源的姿态测量设备,在卫星、导弹、舰船等平台得到广泛应用。对于需在大气层内全天时工作的近地空间平台,如舰船、飞机、导弹、高空气球等,星敏感器面临白天强烈天空背景条件下探测暗弱恒星目标的难题。首先介绍了近地空间全天时星敏感器的基本工作原理;其次介绍了国内外研究现状;然后分析并总结了全天时星敏感器实现的主要技术途径;最后梳理出下一步研究方向。分析结果可为近地空间全天时星敏感器系统的研制提供参考和帮助。     

弹载大视场星惯组合深度融合导航技术

为了降低弹载星惯组合（Stellar-INS）飞行中段对调姿观星的要求，提高星惯组合姿态精度，提出了大视场（LFOV）星惯组合深度融合导航方法。小视场（NFOV）星敏感器输出星矢量为主，大视场星敏感器可同时输出姿态和星矢量信息，分别推导了基于星敏感器输出姿态和星矢量信息的观测方程，分析了星矢量和姿态观测方法之间的关联性。建立了包含星惯安装误差、陀螺误差以及初始平台误差角的星惯组合全误差项模型，基于线性卡尔曼滤波给出了深度融合导航方法。开展了数学仿真验证，分析了不同调姿观星路径约束下，大/小视场星惯组合性能差异。结果表明，大视场星惯组合深度融合导航方法不仅可以降低调姿观星约束要求，还可以实现组合姿态性能提升。     

自适应的光纤布拉格光栅图像寻峰算法

根据实际光谱特征, 提出了自适应的光纤布拉格光栅图像寻峰算法。针对 不同环境物理场及噪声分布下的光栅谱型,该算法能自动检测光谱的带宽和信噪比,自 适应地调整算法的高斯模板带宽大小,提高谱型匹配及滤波效果,从而提高寻峰精度。 将该算法与高斯拟合法、质心法进行对比,分析了其在不同噪声大小及非均匀温度场分 布下光纤布拉格光栅反射光谱的寻峰精度。理论仿真及实际寻峰结果表明,该寻峰算法 具有较强的抗噪能力及谱型适应性,较质心法、高斯拟合法具有显著优势。     

一种新的红外背景抑制滤波算法

结合保护带和Dempster-Shafer(D-S)证据理论,提出了一种新的红外背景抑制滤波算法。首先分析了小目标的特性,论证了小目标在局部背景中呈现出极值性的条件和可能性,并在此基础上采用D-S证据理论计算最佳滤波尺寸。然后在最佳滤波尺寸下,根据保护带的思想进行背景抑制滤波,该算法能够适用不同尺寸的小目标。以全局信噪比增益、局部信噪比增益和背景抑制系数作为算法性能评价标准,实验结果表明,在低信噪比的情况下该算法对典型的不同红外背景具有良好的适用性,能够有效地抑制红外背景并增强目标信息。     

高轨目标掩星成像相位恢复技术研究

高轨目标掩星成像通过观测高轨卫星对恒星的遮掩过程,实现对高轨目标的成像.该方法采用望远镜线性阵列观测高轨目标遮掩恒星过程中恒星亮度变换,获得高轨目标在地面的投影,通过相位恢复方法可计算得到卫星轮廓图样,具有成像分辨力高,设备制造难度小等优点,在高轨目标成像领域具有较好应用前景.本文分析利用掩星成像方法对高轨目标成像的可行性,重点对掩星成像过程的相位恢复方法进行改进,根据掩星成像特点对输入输出算法进行优化,仿真结果表明：改进后的相位恢复方法可显著提高图像恢复质量和掩星成像方法的空间分辨力.     

基于恒星敏感器的仪器星等修正方法

基于恒星敏感器的仪器星等修正方法主要包括星际消光计算（大气层外）与大气消光计算（大气层内）两部分。通过对SKY2000原始星表的恒星星等进行转换计算,修正后星等差一般为0.5星等左右,且与观测仪器的光谱响应有关。     

基于标签多伯努利滤波的衍生目标跟踪算法

针对现有随机有限集(RFS)滤波器在低信噪比环境下对衍生目标跟踪性能严重下降的问题,提出了一种基于Delta扩展标签多伯努利(δ-GLMB)滤波器的改进算法。基于随机集理论和伯努利衍生模型,推导了新的预测方程,并采用了假设裁剪及分组手段和多伯努利近似技术以降低算法的计算量。针对假设增多引起的虚警问题,将多帧平滑思想和算法相结合,利用标签信息对新目标进行回溯处理。仿真结果表明,所提算法能对目标数目进行无偏估计,在低探测概率和强杂波环境下性能明显优于概率假设密度(PHD)算法,计算开销在衍生初始阶段增长快于PHD,目标较分散时低于PHD。     

On suboptimal detection of 3-dimensional moving targets

The author designates matched filters that are completely characterized by the velocity of the target as assumed velocity filters (AVFs). Like most matched filtering techniques where the signal parameters range in a continuum, the AVF must be implemented suboptimally by partitioning the velocity space. The author investigates the possibility of using a signal-to-noise ratio (SNR) loss factor as the criterion for the partition. The loss factor is a measurement of the loss of SNR at the output of the matched filter due to mismatch of filter parameters. In the scenario of detecting a moving satellite from a ground-based sensor, because of the vast sky the sensor has to search, it is important to keep the number of filters minimal. The author shows that, with a fixed loss factor, the number of filters required for coverage increases linearly as the span of the two-dimensional velocity space increases quadratically. The rate of increase is further reduced when the loss factor is made proportional to expected target angular speed     

The Moon as Source for G/T Measurements

For large-aperture antennas, it is customary to utilize radio stars in order to determine the receiving gain to temperature ratio. In the case of small-aperture antennas, which not only have reduced gain but usually higher system noise temperature as well, the y factors obtained from the radio star measurements are so small that the measurement error is intolerable. The moon, on the other hand, provides a power flux density higher by at least one order of magnitude compared to the strongest radio star, and the resulting y factors are usable. G/T ratios determined from moon measurements agree well with expected values.     

Interlaced Kalman filtering of 3D angular motion based on Euler'snonlinear equations

A novel Kalman filtering technique is presented that reduces the mean-square-error (MSE) between three-dimensional (3D) actual angular velocity values and estimated ones by an order of magnitude (when compared with the MSE resulting from direct measurements) even under extremely low signal-to-noise ratio conditions. The filtering problem is nonlinear in nature because the dynamics of 3D angular motion are described by Euler's equations. This nonlinear set of differential equations state that the angular acceleration in one axis is proportional to the torque applied to that axis, and to the products of angular velocity components in the other two axes of rotation. Instead of using extended Kalman filtering techniques to solve this complex problem, the authors developed a new approach where the nonlinear Euler's model is decomposed into two pseudolinear models (primary and secondary). The first model describes the time progression of the state vector containing the linear terms, while the other characterizes the propagation of the state vector containing the nonlinearities. This makes it possible to run two interlaced discrete-linear Kalman filters simultaneously. One filter estimates the values of the state vector containing the linear terms, while the other estimates the values of the state vector containing the nonlinear terms in the system. These estimates are then recombined, solving the nonlinear estimation process without linearizing the system. Thus, the new approach takes advantage of the simplicity, computational efficiency and higher convergence speed of the linear Kalman filter form and it overcomes many of the drawbacks typical of conventional extended Kalman filtering techniques. The high performance and effectiveness of this method is demonstrated through a computer simulation case study     

The fundamental parameters of the central stars of eight WR ring nebulae

We describe work that has recently been completed on deriving the fundamental parameters of eight WR stars through the photoionization modelling of their surrounding nebulae using non-LTE WR flux distributions. The resulting effective temperatures range from 57 000–71 000 K for the WN4-5 stars and <30 000–42 000 K for the WN6-8 stars. The derived stellar parameters are compared with those obtained from stellar emission line modelling. We find good agreement for the hot early WN stars, indicating that the non-LTE WR flux distributions have essentially the correct shape in the crucial far-UV region. We find lower temperatures for the four cooler late WN stars, particularly for the two WN6 stars. For the nebulae surrounding these stars, we find that the model flux distributions produce too much nebular ionization. We suggest that these discrepancies arise because of the lack of line-blanketing in the WR atmospheres. For the WO1 central star of G2.4+1.4, with strong nebular He II 4686 A emission, we derive a temperature of 105 000 K, somewhat less than previous estimates. The positions of our eight WR stars on the H-R diagram are compared with the evolutionary tracks of Maeder (1990) for solar metallicity. In common with previous workers, we find that our derived luminosities are too low, giving an initial mass range of 25–40 M, below that expected for the majority of WR stars.     

Hard Limiting and Sequential Detection Applied to Loran-C

The combination of an antenna, a 100 kHz bandpass filter, a hard limiter, and a sequential detector can supply highly accurate Loran-C data to a digital processor, even under low signal-to-noise-ratio conditions. For such a simple, low-cost receiver, calculations are given for the accuracy of the envelope and phase tracking of the Loran-C signal as a function of the signal-to-noise (Gaussian and atmospheric) ratio, averaging time, and radian speed of the observer with respect to the transmitter. Mentioned are the quasi-noise censoring effects of the hard limiter. Besides the Loran-C application, the hard limiter-sequential detector system can in general be applied for low-cost, synchronous signal detection under poor signal-to-noise ratio.     

星点坐标辅助的全天区三角形星图识别算法

随着当前星敏感器视场（FOV）的增大,探测能力的提高,一帧图中拍摄到的恒星更多。但是受星敏感器光谱范围的限制及空间环境干扰影响,星等测试精度一般不高于0.2 mV。为了充分发挥当前星敏感器视场和探测能力的优势,并避免星等误差的影响,提高全天区星图识别算法在线应用的适用性,提出了一种星点坐标辅助的全天区三角形星图识别算法。该方法采用"全局初步搜索识别—局部精细匹配验证—最优结果选取"的算法思想。首先,根据星敏感器探测到的极限星等范围构建导航星表,选取亮星构建角距星表,既确保了星表的完备性,又有利于充分利用星敏感器的探测能力。然后,在三角形约束条件下进行角距匹配识别,得到一个或多个导航三角形,在该识别环节提出了非线性矢量法查找星表,既提高了定位精度,又能采用单精度数据类型降低存储空间。最后,提出局部天区星点坐标匹配算法进一步消除冗余匹配,同时又识别出视场内更多的观测星,有利于提高识别率和定姿精度。试验结果表明,与其他一些经典的星图识别算法相比,所提算法在识别率和星表容量方面更有优势。识别率可达99.9%,且随着星等的增加,存储容量增加的最少。所提算法更加适于大视场、高星等敏感范围的星敏感器在线应用。     

Signal-to-Noise Ratio in the Bandpass Output of a Discriminator

A formula is derived for the output signal-to-noise power ratio from a limiter-discriminator that is followed by an ideal (rectangular) bandpass filter. This signal-to-noise ratio is shown to be inversely proportional to the difference between the cube of the upper cutoff frequency and the cube of the lower cutoff frequency. The formula commonly utilized by designers for the discriminator output signal-to-noise ratio was derived for the case of a lowpass filter on the discriminator output. The bandpass and low-pass formulas are compared to indicate 1) the advantage of bandpass filtering for the discriminator output, and 2) the error incurred if the designer employs the low-pass formula to evaluate the performance of a bandpass filter design. Finally, the accuracy of a narrow-band approximation for the bandpass formula is evaluated.     

Degradation of Signal-to-Noise Ratio Due to IF Filtering

A receiver for biphase modulated signals using an integrate-and-dump filter is optimum only if the IF filter bandwidth is infinite. Finite IF filter bandwidth results is a performance degradation. Using the predetection signal-to-noise ratio as the performance criterion, a lower bound on this quantity is determined as a function of the ratio (IF filter bandwidth)/(bit rate). The corresponding upper bound on the error probability is also presented.